All Figures

$\begin{figure} \hbox{ \includegraphics[height=9cm,angle=-90]{9506fig1.ps}\hspace{0.3cm} \includegraphics[height=9cm,angle=-90]{9506fig1b.ps} } \end{figure}$ Figure 1: PN XB1832-330 lightcurves of the two observations in the energy ranges 0.3-2 keV and 2-12 keV. The bottom panels show the hardness ratios (counts between 2-12 keV divided by those between 0.3-2 keV) in the two observations. The binning is 1024 s.
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In the text

$\begin{figure} \par\includegraphics[height=8.cm,angle=-90]{9506fig2.ps}\end{figure}$ Figure 2: Ratio between the data and the model when fitting the MOS1, MOS2, and pn spectra of obs I with a double-component continuum (power law, together with a blackbody) absorbed by a partial covering fraction component, which accounts for the global spectral shape of the X-ray emission. The different (and ``opposite'') residuals in the pn (open circles), compared with the MOS1 (stars) and MOS2 (squares), are evident. A similar structured excess is present in the obs II spectrum.
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In the text

$\begin{figure} \par\hbox{ \includegraphics[height=9.cm,angle=-90]{9506fig3.ps}\hspace{0.3cm} \includegraphics[height=9.cm,angle=-90]{9506fig3b.ps} } \end{figure}$ Figure 3: RGS1 and RGS2 XB1832-330 spectra in the two observations, fitted with the continuum model used to fit the broad-band spectra (see text). The bottom panels show the residuals in units of standard deviations. The missing regions in the RGS plots are due to the failed CCDs.
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In the text

$\begin{figure} \hbox{ \includegraphics[height=9.cm,angle=-90]{9506fig4.ps}\hspace{0.3cm} \includegraphics[height=9.cm,angle=-90]{9506fig4b.ps} } \end{figure}$ Figure 4: RGS1 and RGS2 XB1832-330 spectra in the two observations, limited to the wavelenght region around the Oxygen edge. In the left panel, the excesses just above 23 Å could be due to the O III emission line, but it is less than 2 $\sigma$ from the continuum and the statistics hampers a more detailed analysis.
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In the text

$\begin{figure} \hbox{ \includegraphics[height=9.cm,angle=-90]{9506fig5.ps}\hspace{0.3cm} \includegraphics[height=9.cm,angle=-90]{9506fig5b.ps} } \end{figure}$ Figure 5: Lomb-Scargle periodograms of the two XMM-Newton observations, 2006 September on the left and 2006 October on the right.
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In the text

$\begin{figure} \par\includegraphics[height=6.5cm,angle=0]{9506fig6.eps}\end{figure}$ Figure 6: Lightcurves of the two EPIC observations folded on the periods P = 9170 s (Obs I, upper panel) and P = 18 616 s (Obs II, lower panel). Phase zero is arbitrary.
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In the text

$\begin{figure} \par\includegraphics[height=8.75cm,angle=0]{9506fig7.ps}\end{figure}$ Figure 7: Distribution of the 46 detected X-ray sources over the EPIC focal plane. The central CCD is empty since it was operated in Small Window mode and no source detection was performed on its data. Numbers mark the 46 sources listed in Table 4.
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In the text

$\begin{figure} \par\includegraphics[height=8.75cm,angle=-90]{9506fig8.ps}\end{figure}$ Figure 8: Colour-colour diagram of the detected sources. Open circles mark the simulated colours (obtained with an absorbed power-law spectrum, assuming different photon indexes and absorption columns). From top to bottom the photon index is 1, 2, and 3; from left to right different column densities have been assumed: 0.1, 0.5, 1, 3, 6, $9\times 10^{21}$ cm^-2.
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In the text

$\begin{figure} \hbox{ \includegraphics[height=9cm,angle=-90]{9506fig1.ps}\hspace{0.3cm} \includegraphics[height=9cm,angle=-90]{9506fig1b.ps} } \end{figure}$	Figure 1: PN XB1832-330 lightcurves of the two observations in the energy ranges 0.3-2 keV and 2-12 keV. The bottom panels show the hardness ratios (counts between 2-12 keV divided by those between 0.3-2 keV) in the two observations. The binning is 1024 s.
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$\begin{figure} \par\hbox{ \includegraphics[height=9.cm,angle=-90]{9506fig3.ps}\hspace{0.3cm} \includegraphics[height=9.cm,angle=-90]{9506fig3b.ps} } \end{figure}$	Figure 3: RGS1 and RGS2 XB1832-330 spectra in the two observations, fitted with the continuum model used to fit the broad-band spectra (see text). The bottom panels show the residuals in units of standard deviations. The missing regions in the RGS plots are due to the failed CCDs.
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$\begin{figure} \hbox{ \includegraphics[height=9.cm,angle=-90]{9506fig4.ps}\hspace{0.3cm} \includegraphics[height=9.cm,angle=-90]{9506fig4b.ps} } \end{figure}$	Figure 4: RGS1 and RGS2 XB1832-330 spectra in the two observations, limited to the wavelenght region around the Oxygen edge. In the left panel, the excesses just above 23 Å could be due to the O III emission line, but it is less than 2 $\sigma$ from the continuum and the statistics hampers a more detailed analysis.
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$\begin{figure} \hbox{ \includegraphics[height=9.cm,angle=-90]{9506fig5.ps}\hspace{0.3cm} \includegraphics[height=9.cm,angle=-90]{9506fig5b.ps} } \end{figure}$	Figure 5: Lomb-Scargle periodograms of the two XMM-Newton observations, 2006 September on the left and 2006 October on the right.
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$\begin{figure} \par\includegraphics[height=6.5cm,angle=0]{9506fig6.eps}\end{figure}$	Figure 6: Lightcurves of the two EPIC observations folded on the periods P = 9170 s (Obs I, upper panel) and P = 18 616 s (Obs II, lower panel). Phase zero is arbitrary.
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$\begin{figure} \par\includegraphics[height=8.75cm,angle=0]{9506fig7.ps}\end{figure}$	Figure 7: Distribution of the 46 detected X-ray sources over the EPIC focal plane. The central CCD is empty since it was operated in Small Window mode and no source detection was performed on its data. Numbers mark the 46 sources listed in Table 4.
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$\begin{figure} \par\includegraphics[height=8.75cm,angle=-90]{9506fig8.ps}\end{figure}$	Figure 8: Colour-colour diagram of the detected sources. Open circles mark the simulated colours (obtained with an absorbed power-law spectrum, assuming different photon indexes and absorption columns). From top to bottom the photon index is 1, 2, and 3; from left to right different column densities have been assumed: 0.1, 0.5, 1, 3, 6, $9\times 10^{21}$ cm^-2.
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